Cosmology without having General Relativity (GR) can be formulated from Newton’s theory [1]}, [2]}, [3]}, [4]}, [5]}, [6]}, [7]}. The Friedmann equation that describes the expansion of the Universe has a form of kinetic part \(\dot{a}^2\)  and a potential-like part \(V(a)\)  [8]}, where \(a\)  is the scale factor of the universe. [9]} derives the Friedmann equations from a symmetry. In particular, while one frame introduces a homogeneous expansion, where Hubble law is valid with respect to any point in the universe, [9]} shows that the homogeneity of the universe emerges from a basic
symmetry on the Newton's Second Law (NSL) which allows to introduce a uniform acceleration in space, but not
constant in time. In order to obtain a symmetry of the Newtonian equations of motion, the Newtonian potential is
also transformed accordingly. Two transformations are involved in the symmetry: One is transforms the position to an accelerated system, and the other one adds a linear contribution to the gravitational potential. The transformation in position is actually the equivalence principle of Einstein and the addition of the linear contribution produce a constant gravitational field. Those two effects cancels each other and yields the Freidmann equations.
